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Detectors and Analog Electronics. Bill Crain The Aerospace Corporation 310-336-8530 [email protected]. Introduction. Design Overview Requirements Flowdown Detector Specification Signals, Noise, and Processing Board Descriptions Interface Block Diagram Power Consumption Trade Studies - PowerPoint PPT Presentation
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Cosmic RAy Telescope for the Effects of Radiation
Detectors and Analog Electronics
Bill CrainThe Aerospace Corporation
Cosmic RAy Telescope for the Effects of Radiation
Introduction• Design Overview• Requirements Flowdown• Detector Specification• Signals, Noise, and Processing• Board Descriptions• Interface Block Diagram• Power Consumption• Trade Studies• Summary
Cosmic RAy Telescope for the Effects of Radiation
Detector Electronics Design Overview• Detector electronics comprised of two board designs
– Detector Boards in Telescope assembly– Analog Processing Board (APB) in E-box
• Heritage approach from Polar CEPPAD/IPS unchanged from proposal– Linear pulse processing system utilizing Amptek hybrids– Circuits re-designed for CRaTER requirements
• Functional requirements summary– Measure LET of high LET particles in thin detectors– Measure LET of low LET particles in thick detectors– Provide good resolution for TEP effects– No fast timing requirements– Robust to temperature drift and environments
Cosmic RAy Telescope for the Effects of Radiation
Analog Signal Flow Diagram
• Single fixed gain, linear transfer function• All detector channels use same topology
– Differences in preamp input transistor, detector biasing, and gain settings are made to optimize thin and thick channels
UnipolarLinear Output
Leading-edgeTrigger
dv/dt &Pole-Zero
Cancellation
ShapingAmp
Amp
BaselineRestorer
Preamp
Low-levelTrigger
SiliconDetector
BiasNetwork
TestPulser
Buffer
Cosmic RAy Telescope for the Effects of Radiation
Requirements FlowdownElectronics reqs. derived from Level 2 reqs. and detector sims.Electronics Req. Thin Det. Thick Det. Level 2 Req. Affectivity
Amplifier strings 3 3 TEP analysis System design
Stability / drift 0.1% (1 bit) 0.1% (1 bit) Resolution Preamp, bias network, baseline restorer
Max. Energy Deposit 1 GeV for Fe 100 MeV for H+ LET spectrum range
Preamp range, closed-loop stability
Low E Threshold 2 MeV 200 keV LET spectrum range
Gain, baseline restorer, shaping time
Noise (rms) < 500 keV (1/2bit)
< 50 keV (1/2bit) Resolution Preamp, shaping time, thermal
Max. Singles Rate 10 kHz 10 kHz ESP events Shaping time, preamp time constant
Output Linear Linear Resolution Output amplifier
Internal Calibration 1000:1 1000:1 Operations Test pulser
Cosmic RAy Telescope for the Effects of Radiation
Detector Specification (1)• Micron Semiconductor Limited
– Lancing Sussex, UK
• 20 years experience in supplying detectors for space physics– CEPPAD, CRRES, WIND, CLUSTER, ACE, IMAGE, STEREO,
and more…
• Detector Type– Ion-implanted doping to form P+ junction on N-type silicon– Very stable technology– Advantages to science include good carrier lifetime, stable to
environmental conditions, and thin entrance windows
Cosmic RAy Telescope for the Effects of Radiation
Detector Specification (2)• Circular detectors having active area of 9.6 cm2
• Two different detector thicknesses: thin and thick– note: state-of-the-art is 20um for thin and 2,000um for thick detectors
• Guard ring on P-side to improve surface uniformity• Very thin dead layers (windows) reduce energy loss, lower
series resistance, and reduce noise
Guard P+ Contact Guard
Active Volume(depletion region)
P+ window
N window
0.1 um
0.1 um
140 um thin;1,000 um thick
35 mm, diam.
N contact
E-field
Cosmic RAy Telescope for the Effects of Radiation
Detector Specification (3)
• Detector drawings (Micron)
Guard ring
Al. contact grid reduces surface resistivity
Al. contact plane
Cosmic RAy Telescope for the Effects of Radiation
Detector Specification (4)
• ISO9001 – Full traceability and serialization– Travelers maintained
• Verification and test prior to detector shipment– Random vibration test– Thermal cycling and thermal vacuum– Stability
• Test criteria– Leakage current– I-V characteristic– Alpha resolution / pulser noise measurement (final test)
Cosmic RAy Telescope for the Effects of Radiation
Proton Energy Deposition Simulations Reference:M. Looper
Thin 150MeV incident E Thick 150MeV incident E
Thin 1000MeV incident E Thick 1000MeV incident E1 GeV Protons
1
10
100
1000
10000
0.01 0.1 1 10 100
Deposited Energy (MeV)
Even
ts
Detector 2Detector 4Detector 5
20,000 incident protonsThick detectors (1000 um)
1 GeV Protons
1
10
100
1000
10000
0.01 0.1 1 10 100
Deposited Energy (MeV)
Even
ts
Detector 1Detector 3Detector 6
20,000 incident protonsThin detectors (140 um)
150 MeV Protons
1
10
100
1000
10000
0.01 0.1 1 10 100
Deposited Energy (MeV)
Even
ts
Detector 2Detector 4Detector 5
20,000 incident protonsThick detectors (1000 um)
150 MeV Protons
1
10
100
1000
10000
0.01 0.1 1 10 100
Deposited Energy (MeV)
Even
ts
Detector 1Detector 3Detector 6
20,000 incident protonsThin detectors (140 um)
Nom
inal
Thr
esho
ld
Nom
inal
Thr
esho
ld
GEANT4
Cosmic RAy Telescope for the Effects of Radiation
Iron Energy Deposition Simulation
Reference:J.B. Blake
Cosmic RAy Telescope for the Effects of Radiation
Signal Characteristics
Detector Min Signal Max Signal Collection Time
DetectorCapacitance
FeedbackCapacitance
Thin 555E3 e-h pairs(88 fC)
275E6 e-h pairs(44 pC)
3 nsec e-drift9 nsec h-drift
700 pF 10 pF
Thick 55E3 e-h pairs(8.8 fC)
27.5E6 e-h pairs(4.4 pC)
38 nsec e-drift115 nsec h-drift
100 pF 1.0 pF
qμnNe(t)E qμpNh(t)E
PreAmp
Cdet
CFB
RFB
CFB (Ao) >> Cdet
AoVpk = Qtot/CFB
Cosmic RAy Telescope for the Effects of Radiation
Signal Processing (1) • Combined dynamic range of thin/thick pair is 5,000 • Thin threshold to provide overlap with thick range• Thin Detector Signal
– Preamp input stage designed for 97% charge collection• High gain input jFET to raise dynamic input capacitance• 4% drift in operating point will result in 0.1% in output peak (< 1 bit)
– Large feedback capacitance needed to handle Fe deposit• Preamp compensation to maintain closed-loop stability
• Thick Detector Signal– Not as sensitive to detector capacitance– Design for low noise to maintain reliable 200 KeV low threshold
and achieve < 1-bit resolution
Cosmic RAy Telescope for the Effects of Radiation
Noise Model (1)
Reference:Helmuth SpielerIFCA Instrumentation Course Notes2001
Detector Input Capacitance
Leakage Current
Shunt Resistance
Series Resistance
Preamp noise (ena)
Thin 700 pF Det.160 pF jFET+stray
200 nA @ 20C800 nA @ 35C
260 kohm 100 ohms 0.6 nV/√Hz
Thick 100 pF Det10 pF jFET+stray
200 nA @ 20C800 nA @ 35C
260 kohm 100 ohms 2.0 nV/√Hz
+ input cap.
T=peaking timeF=shaping factors
Cosmic RAy Telescope for the Effects of Radiation
Noise Model (2)
Optimum
Cosmic RAy Telescope for the Effects of Radiation
Signal Processing (2)
• Noise dominated by detector leakage and input jFET• Shaping time for both thin and thick detectors set at thick
optimum point– ~1 usec– Compatible with A/D signal acquisition timing– 3-pole gaussian shaping improves symmetry and 2-complex
poles shortens tail
• Shaping reduces noise but also impacts signal level – S/N at thick detector threshold for this design ~ 4– Translates to a noise occupancy in the coincidence window of <
0.1% for time period not greater than shaping time
Cosmic RAy Telescope for the Effects of Radiation
Signal Processing (3)
• Other factors affecting noise performance– Bias resistor sized to minimize voltage drop (i.e., maintain
stable operating point)– Detector shot noise doubles every 8 C– Beneficial to operate cold; preferably below 20 C
Cosmic RAy Telescope for the Effects of Radiation
Signal Processing (4)
• Pileup is rare due to low event rate and relatively short shaping time– Exception: occasional periods of high ESP flux
• Leading edge trigger technique causes timing uncertainty but coincidence window is large by comparison– Amplified low-level discriminator available to reduce walk
• Ballistic deficit is not an issue due to short collection times relative to peaking time of shaper
• Output voltage scaled for A/D input specifications
Cosmic RAy Telescope for the Effects of Radiation
Detector Board
• Thin/thick detector pair use same design topology
• Signal collected on P-contact• Negative bias• Guard signal shunted to
ground• No guard leakage noise• AC coupling to isolate DC
detector leakage current• Low noise / high gain JFET
input stage
BiasNetwork
Test Input&
FeedbackNetwork
Negative Bias
Test Pulser
Feedback
Signal
P-contactG G
N-contact
Active Volume
JFET
BiasNetwork
Cosmic RAy Telescope for the Effects of Radiation
Analog Processing Board
• Single board in E-box contains 3 thin and 3 thick detector processing channels
• Flight proven pulse processing components– Amptek A250 preamp hybrid utilizing external jFET on detector
board– Shaping amps use Amptek A275 for active filtering– Baseline restorer, Amptek BLR1, compensates for baseline shifts on
interface to A/D
• Pole-zero cancellation circuit for correcting preamp pulse decay to eliminate undershoot
• Test pulser injects ΔQ at preamp input jFET
Cosmic RAy Telescope for the Effects of Radiation
Analog Interface Block Diagram
Bias
Temperature (uA/K)
Thin detector signalThin detector feedback
Thin test input
Returns
Detector Board 2(same)
Detector Board 3(same)
Power & Returns
Unipolar Signals
3 thin, 3 thickLow-level Triggers
Pulser Level (thick)Pulser Level (thin)
Det. Bias& Returns
Temperatures
MIT
1000 um
140 um
Thick detector signalThick detector feedback
Thick test input
Pulser Trigger
3 thin, 3 thick
Telescope Assembly(3 Detector Boards) Analog Processing Board
Aerospace
PHA System
Digital Processing
Cosmic RAy Telescope for the Effects of Radiation
Power Estimate
Current Est. (mA) 10% Uncertainty Current Est. (mA) 10% Uncertainty24-May-05 24-May-05 24-May-05 24-May-05
+6V Analog 27.000 29.700 61.800 67.980 88.800 97.680
-6V Analog 0.000 0.000 41.800 45.980 41.800 45.980
+5V Digital 0.000 0.000 1.000 1.100 1.000 1.100
-100V Thin Det Bias 0.030 0.033 0.000 0.000 0.030 0.033
-300V Thick Det Bias 0.075 0.083 0.000 0.000 0.075 0.083
Power Est. (mW) 10% Uncertainty Power Est. (mW) 10% Uncertainty Total Est. (mW) Total Max. (mW)
Total Load 187.5 206.25 626.6 689.26 814.1 895.51
Total Est. (mA) Total Max. (mA)Analog Processing Board
Power SourceDetector Boards (total for 3 boards)
Total estimated power dissipation is < 1 Watt
Cosmic RAy Telescope for the Effects of Radiation
Trade Studies
• Determine if one detector board can be implemented instead of three
• Determine if A250 device should be located on detector board
• Determine sensitivity of APB to detector performance– Want to avoid rework of APB when selecting/changing detectors
during development
• Determine how best to isolate chassis noise from detectors and preamp
Cosmic RAy Telescope for the Effects of Radiation
Summary
• Detectors are well-established technology from experienced supplier
• Detector electronics design meets requirements of Level 2 mission and satisfies energy deposition levels determined by detector/TEP simulations
• Trade studies in progress